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Gravitational Collapse

Abstract

RECENTLY there has been renewed interest in the ultimate fate of the gravitational collapse of large masses. From the early work of Chandrasekhar1, Oppenheimer and Volkoff2, and the more recent work of others3, it is clear that for a relativistic gas there is a critical spherical mass of Mc ∼ 1 M⊙, where M⊙ is the mass of the Sun. In any relativistic degenerate mass of M > Mc, no matter what radius it has, the gravitational field everywhere exceeds the outward force exerted by the pressure gradient. No static equilibrium configuration is possible, and hence the mass continuously collapses.

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References

  1. Chandrasekhar, S., Stellar Structure (University of Chicago Press, 1939).

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  2. Oppenheimer, J. R., and Volkoff, G. M., Phys. Rev., 55, 374 (1939).

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  3. Harrison, B. K., Wakano, M., and Wheeler, J. A., La Structure et l'Evolution de l'Univers (Brussels: Stoops, 1958). Wheeler, J. A., Relativity and Gravitation, edit. by Chin, H. Y., and Hoffmann, W. F. (New York, Benjamin, 1963). See also review article: Chiu, H. Y., Ann. Phys., 26, 364 (1964).

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  4. Tolman, R. C., Relativity Thermodynamics and Cosmology, 252 (Oxford, Clarendon Press).

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HARRISON, E. Gravitational Collapse. Nature 204, 1179–1180 (1964). https://doi.org/10.1038/2041179a0

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